Nonpulsating Stars and the Populations i and II Instability Strips
With specially computed detailed tables of equations of state and opacities, the instability strips for delta Scuti stars and Cepheids of Population I and RR Lyrae and W Virginis stars of Population II have been computed. Uncertainties in the observed strip locations and sometimes in the mode of the observed pulsations do not allow high accuracy in fixing helium contents or the variables masses. Nevertheless, if masses close to those given by evolutionary theory are used, the helium content in Population II objects is likely less than Y=0.25. For Population I, Y can be more than 0.3; but if a given star has Y less than abeut 0.25, it can appear in the dwarf and classical Cepheid strips as nonpulsating.
- Research Organization:
- University of California, Los Alamos Scientific Laboratory, Los Alamos, New Mexico
- Sponsoring Organization:
- USDOE
- NSA Number:
- NSA-29-021840
- OSTI ID:
- 4348669
- Journal Information:
- Astrophysical Journal, Journal Name: Astrophysical Journal Vol. 184; ISSN 0004-637X
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
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